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List of Figures

1.1 Shape of s, p, d, f electron orbitals
1.2 Periodic table of elements
1.3 First ionization potentials and electron affinities
1.4 Hybrid orbitals of carbon
1.5 Different types of molecular bonds
1.6 An example of σ and π bonds
1.7 Origin of the band structure of a solid
1.8 The Fermi level and the different types of solid
1.9 Structure of interstellar dust candidates
1.10 Appearance of various minerals
1.11 Absorption, scattering and emission
1.12 Effect of an electromagnetic wave on a dielectric
1.13 Amplitude of a forced harmonic oscillator
1.14 Idealized optical constants
1.15 Molecular transitions
1.16 Dielectric functions of different materials
1.17 Illustration of the extinction paradox
1.18 Mie, Rayleigh and geometric optics regimes
1.19 Cross-sections of silicate and graphite grains
1.20 Oblate and prolate spheroids
1.21 Absorption cross-sections of grain aggregates computed with DDA
1.22 Stokes parameters
1.23 The three types of grain-induced polarization of light
1.24 Phonon modes
1.25 Heat capacities.
1.26 Emissivity of grains at thermal equilibrium with the radiation field
1.27 Planck averages of graphite and silicates
1.28 Diffuse Galactic ISRF
1.29 Grain equilibrium temperatures
1.30 Temperature fluctuations of grains with different radii
1.31 Temperature fluctuations of grains with different starlight intensities
1.32 Stochastically heated grains
1.33 Transition radius for stochastically heated grains
1.34 Photon and electron energy densities
1.35 Collisional heating rate
2.1 Early ISM and IR astronomy
2.2 Absorbance of Earth’s atmosphere
2.3 Airborne observatories
2.4 All sky maps
2.5 Analysis of the Stardust mission
2.6 First evidences of interstellar dust
2.7 The pioneers
2.8 First detection of UIBs
2.9 Désert et al. (1990) dust model
2.10 Panchromatic dust observables
2.11 Galactic extinction curves
2.12 MIR extinction
2.13 X-ray edges
2.14 Polarized extinction and DIBs
2.15 Galactic diffuse ISM SED
2.16 Solar abundances
2.17 Depletion variations within the MW
2.18 MW dust composition inferred from depletions
2.19 Presolar grains in meteorites
2.20 Micrometeorite collection in Antarctica
2.21 NASA Ames PAH experiment
2.22 Laboratory measurement of silicate opacities
2.23 Size distribution of several dust models
2.24 Model opacity and emissivity
2.25 THEMIS fit of the Galactic constraints
2.26 IR approximation of the opacity
2.27 Effect of U on the SED
3.1 Moments of the specific intensity
3.2 The radiative transfer equation
3.3 Solution to the radiative transfer equation for an isothermal cloud, without scattering
3.4 Escaping radiation from a spherical cloud
3.5 Escaping SED from clumpy spherical clouds
3.6 Principle of Monte-Carlo radiative transfer
3.7 Drawing photons in a Monte-Carlo radiative transfer model
3.8 Drawing scattering angles in a Monte-Carlo radiative transfer model
3.9 Spatial distributions of the clumpy radiative transfer model
3.10 Random photon path within a clumpy medium
3.11 Total SED from the clumpy radiative transfer model
3.12 MBB fitting
3.13 Phenomenological mixing of physical conditions
3.14 Effect of the ISRF hardness on the SED
3.15 Degeneracy of the grain size and ISRF distributions
3.16 SED fit with the Draine & Li (2007) starlight intensity distribution
3.17 Comparison of different SED models
3.18 Stellar isochrones
3.19 Evolution of stellar SEDs as a function of time
3.20 Multiphase SEDs of galaxies
3.21 Matryoshka effect demonstrated on the LMC
3.22 Hubble-de-Vaucouleurs galaxy morphology diagram
3.23 Visible-range image of three nearby galaxies
3.24 Principal sources of contaminations encountered when modeling SEDs
3.25 Radiative transfer modeling of NGC 4565
3.26 Dust mass discrepancy in the LMC
3.27 Effect of a blast wave on the grain size distribution
3.28 Grain size distribution in four dwarf galaxies
3.29 Extinction curves of low-metallicity environments
3.30 MIR spectra of galaxies
3.31 Vibrational modes of PAHs
3.32 Laboratory and theoretical PAH spectra
3.33 Empirical calibration of UIB profiles
3.34 MIR spectral fitting methods
3.35 PAH and small grain templates
3.36 Diversity of MIR spectra among and within galaxies
3.37 PAH band ratio correlations inside and among galaxies
3.38 Theoretical MIR band ratio variations
3.39 Calibration of PAH ratio diagnostics
3.40 PAH band ratio as diagnostics of the physical conditions
3.41 Effect of ISRF hardness on PAH strength
3.42 Effect of metallicity on the PAH strength
3.43 Submillimeter excess in NGC 1569
3.44 Spatially-resolved submm excess in the LMC
3.45 AKARI 9 μm map of λ-Orionis
3.46 AME correlation with ionized PAHs in λ-Orionis
3.47 Cooling function of the ISM at Solar metallicity
3.48 Photoelectric heating in PDRs
3.49 Neutral ISM phase diagram
3.50 H2 formation on grain surface
3.51 Structure of a PDR
3.52 Comparison of visual extinctions in 30 Doradus
3.53 Metallicity effect on the CO-dark gas
3.54 Molecular gas pressure in the center of M 83
4.1 The interstellar dust lifecycle
4.2 Average nuclear binding energies per nucleon
4.3 Schematic representation of stellar evolution
4.4 Initial mass functions
4.5 Parametric star formation histories
4.6 Nucleosynthesis origin of the main elements
4.7 Solar metallicity elemental stellar yields
4.8 Spatially-resolved SED fits in N44 and N66
4.9 Dust-to-gas mass surface density relation in N44 and N66
4.10 Grain growth timescales
4.11 Lifetimes of small grains in a radiation field
4.12 Carving out of PAHs by UV photons in N11
4.13 Thermal and kinetic sputtering times of silicates and carbon grains
4.14 Evidence of thermal sputtering in elliptical galaxies
4.15 Effects of dust evolution on the SEDs of galaxies.
4.16 Dust evolution tracks for a MW-like galaxy
4.17 Effects of SFH-related parameters on dust evolution
4.18 Effects of tuning parameters on dust evolution
4.19 Dustiness-metallicity relation fitted with a dust evolution model
4.20 Empirical estimates of dust evolution timescales as a function of metallicity
4.21 Evolution of the mass fraction of small a-C(:H) grains with metallicity and starlight intensity
4.22 The potential of quiescent very-low-metallicity galaxies to understand the origin of small a-C(:H) grains
5.1 Venn diagram to demonstrate Bayes’ rule
5.2 Simulation of the measure of a stellar flux to compare Bayesian and frequentist methods
5.3 Bayesian and frequentist solutions to the problem of Fig. 5.2
5.4 The benefits of using an informative prior
5.5 Flux measures with a non-linear detector
5.6 Markov Chain Monte-Carlo algorithms
5.7 Importance of the choice of the Metropolis-Hastings proposal distribution
5.8 Post-processing of the MCMC of a sample of sources
5.9 MCMC statistics of a sample of sources
5.10 Demonstration of the use of posterior predictive p-values
5.11 Bayesian and frequentist hypothesis testing
5.12 The probability pioneers
5.13 The frequentist promoters
5.14 The Bayesian resistance
5.15 Three figures of modern epistemology
5.16 Bayes factors and parsimony
5.17 Example of hierarchical Bayesian SED fits
5.18 Posterior distributions with standard and hierarchical Bayesian methods
5.19 Comparison of least-squares, standard Bayesian and HB methods
5.20 Solving the emissivity-index-temperature degeneracy of MBBs with a HB model
5.21 Demonstration of the effect of the prior in a HB model
5.22 The holistic approach: inclusion of external parameters into the prior
A.1 Spectral domains represented over the SED of a nearby galaxy
C.1 Most common coordinate systems
C.2 Two ways of slicing the πs
C.3 Methods for drawing random numbers from arbitrary distributions
D.1 Nerdy allegory of my collaboration network

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